adsabs/AstroCLIMB huggingface dataset:
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: An illustration of the process by which the surface of the sphere is constructed. Starting from an icosahedron on the left, triangular faces are continually subdivided. Finally, the points are normalized to generate a uniformly sampled sphere.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Same as Figure 6 but for the F775W filter.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Same as Figure 6 but for the F555W filter.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Same as Figure 6 but for the F658N filter.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Continuation of Figure 9.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Continuation of Figure 7.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: CMDs of Gaia19fct. Top left: r vs. g − r diagram based on the ZTF (circle) and RC80 (star) data. Top right and middle left: V vs. V − I and V vs. V − R diagrams based on HOYS data. Middle right: W1 vs. W1 − W2 diagram based on NEOWISE data. Bottom left and right: REM H vs. J − H and H vs. H − K diagrams.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Observed [Fe II] line ratios for Gaia19fct. Dotted red, dashed orange, dashed–dotted green, and dashed–triple-dotted blue lines present models with T  e  = 3000, 5000, 10,000, and 20,000 K, respectively. Gray horizontal lines and ticks represent the observed line ratios and uncertainties.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Best-fit results of Mg I 1.574, Mg I 1.575, and Fe I 1.580 μm. The black line shows the error-weighted mean spectrum of Gaia19fct. Red and blue lines present disk and stellar rotational profiles, respectively.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption:  H- and K-band spectra of Gaia19fct observed on 2020 November 19 (black), 2020 November 23 (light gray), and 2022 March 17 (dark gray). Telluric correction of the second observation (light gray) was not perfect; therefore, emission profiles remained at the edge of each band, especially longer than 2.38 μm. Different colors indicate different spectral lines.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Observed Brackett series of Gaia19fct. Gray, red, and blue lines represent the data observed on 2020 November 19, 2020 November 23, and 2022 March 17, respectively.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Excitation diagram of H2.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Observed H2 lines in 2020 November. The part where the telluric correction is not perfect is missing, e.g., 1–0 S(3) 1.958 μm.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Detected metallic absorption lines in 2020 November.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: [Fe II] emission lines observed in Gaia19fct. Black and blue lines present the spectrum observed in 2020 November and 2022 March, respectively.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Baseline SED model (black line) and variations summarized in Table 4. Varying the disk scale height has a large impact on the SED at the wavelengths covered by Spitzer/IRS.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Spitzer/IRS spectra probing water vapor in the inner disk (Pontoppidan et al. 2010) next to ALMA high-resolution images tracing the outer dust disk emission (Long et al. 2019). Note that the IRS spectrum of DK Tau includes emission from the disks around the A and B components but B contributes < 10% to the broadband mid-infrared flux (McCabe et al. 2006).
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Left panels: best-fit model (black dotted line) superimposed on the continuum-subtracted spectrum of DK Tau (colored line). The light blue shaded regions are those that contribute to the χ 2 calculation in fitting the water spectrum. Right panels: Bayesian probability distributions for the column density (top), emitting radius (middle), and gas temperature (bottom) with the best-fit parameters as blue dashed lines and the 68% confidence intervals as gray-shaded regions.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Continuum-subtracted portion of the Spitzer/IRS spectrum of DK Tau (black) showing the three water bands used in Banzatti et al. (2020) to measure the water-to-organics line ratio. The simulated JWST/MIRI spectra (colored lines, Section 4) highlight that each band includes multiple H2O transitions, a vertical dotted line shows the strongest one for which the flux is reported in the paper.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: H2O/HCN flux ratio vs. dust disk radius and best-fit relation (dashed line) from Banzatti et al. (2020). Our selected sources are highlighted: DK Tau A and IQ Tau cover the extremes of the relation while BP Tau is in the middle.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Continuum-subtracted spectra for DK Tau, BP Tau, and IQ Tau. The light blue shaded regions (hereafter referred to as selected-λ region) include strong water emission uncontaminated by other known atomic or molecular line, and as such, are selected to fit the water spectrum (see Section 3).
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: JWST/MIRI simulated disk spectra. The Disk A spectra are colored blue, Disk B is orange, and Disk C is red. Note that Disk C consistently has a greater flux than Disk A or B at all water lines.
Paper: Testing the Retrieval of Inner Disk Water Enrichment with Spitzer/IRS and JWST/MIRI
Authors: Mackenzie M. James, Ilaria Pascucci, Yao Liu, Andrea Banzatti, Sebastiaan Krijt, Feng Long, Inga Kamp
Figure caption: Portion of the best-fit models (black dotted line) superimposed on the continuum-subtracted spectra of the simulated disks (colored line).
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: HST F475W images of the 14 low-confidence sources in our sample, overlaid with FIRST 1.4 GHz contours in the left panel and zoomed-in to highlight the optical morphology of the galaxy in the right panel. All images are centered on the galaxy with north up and east to the left. The restoring beam of the radio map is depicted as a hatched ellipse on the lower-right corner. The radio contours are (−3, 3, 6, 12, 24, 48, 96,...)×rms of each image, where the values of the rms are listed in Table 3. The scale bar in the lower-left corner of each panel indicates the proper distance at the redshift of each object.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Two-dimensional bulge–disk decomposition using GALFIT of 16 of the 18 high-confidence sources in our sample. The left column shows the surface brightness profile of the data (open circles with error bars), Sérsic bulge component (red), exponential disk component (blue), and total (bulge + disk) model (purple). The ﹩{\chi }_{\nu }^{2}﹩ from GALFIT is shown in the lower-left corner. The lower panel gives the residuals between the data and the model. The right three columns show the original data, best-fit total model, and residuals, respectively. All images are displayed on a log stretch.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Relative position angle (ΔPA) between the radio lobes and the minor axes of the host galaxy (a) disk and (b) bulge. The upper panels show the correlation between ΔPA and bulge-to-total ratio (B/T), where the color code indicates the bulge Sérsic index (n). The lower panels give the distribution of ΔPA in bins of 30°.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption:  M halo−M * relation for the SAM (middle), and as predicted by our GNN, Mangrove (upper). For the 99% of points closest to the median M halo−M * relation, points are plotted as a histogram with logarithmic coloring, whereas the remaining outliers are plotted as points. The outliers are regressed to a remarkable precision, especially for trees with M * way above the median M halo−M * relation. As can be seen comparing the low M  h , M * region, the Gaussian loss allows Mangrove to give up on some low-mass galaxies. This limit is indicated by a dashed black line. Figure 13 in Appendix D shows the same relation for all targets.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Relation between halo masses and target parameters for all targets for both the SAM and Mangrove predictions, in a style similar to that shown in Figure 9, with outliers clearly marked. We furthermore show general trends in the right column, where the dashed and solid lines show the medians and the shaded areas show the 16th and 84th percentiles for the parameter in question for both the SAM and Mangrove. Here, we immediately see the source of some of the errors; for example, the inability of Mangrove to accurately capture the two diverging branches in the SFR.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: In the first column, we show distributions of logarithmic uncertainties. In the second column, we show distributions of pulls/z-scores ﹩\tfrac{{\rm{\Delta }}y}{\hat{\sigma }}﹩, and a unit Gaussian to guide the eye, along with annotations of metrics concerning the pull distributions. The third column shows the relationship between predicted values and uncertainties, along with a red dashed line indicating their median relationship, as well as being annotated with a Pearson correlation coefficient. The fourth and final column shows the relationship between the residuals and the predicted uncertainties, with a clear broadening as one goes toward higher predicted uncertainty.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Same as Figures 3 and 6, but using cuts where only the 50% lowest variance predictions, as predicted by Mangrove, are included. As can be clearly seen, Mangrove does significantly better, even though it tends to avoid regions that are information-poor, like the massive black hole region (M BH > 6.1).
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Relation between M halo and target parameter residuals with respect to the median of the target parameters in M halo bins. 20 bins are used. This is a separate but distinct way of visualizing the main points in Figure 13, i.e., that the dispersion is quite accurate for all parameters but SFR and SFR100. There is thus hope for producing a full galaxy property hyperplane with Mangrove or a similar GNN-based method.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Residual for all targets, along with linear (a*x+b) fits. Each window is annotated with the slope (a) and the intercept (b) of the residual—residual relation in question. The plot is made with the corner package (Foreman-Mackey 2016).
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: The difference between the M */M halo and the median value of M */M halo for halo-galaxy pairs in bins of halo mass bin plotted as a function of the NFW concentration parameter of the halo. The dashed lines show the medians and the shaded areas show the 16th and 84th percentiles. The left panel shows the relationship for the SC-SAM, the middle panel shows that for Mangrove, and the rightmost panel shows a comparison between the two. Equal bin widths are chosen for comparison with Figure 12 in G21.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Same as Figures 3 and 6, but for regressing using only information from the final halo. We see a general decline in performance compared to using the full merger tree, although median relations are improved, and the SFR is slightly better when predicting SFR > 0.2. A single node is still technically a graph; however, no graph structure is used, so the GNN label may be slightly misleading.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Same as Figures 3 and 6, but where the differences are taken between two different runs of the SC-SAM with nothing changed but the random seeds. The numbers are not exactly the same as those in Table 1, since those are the mean of the metrics of different SAM runs.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption:  M-band spectra of the MYSO sample on optical depth scale. A zoom in on the OCS ice band is shown in the right panels. The OCS band is fitted with a single Gaussian. To this are added the Gaussian and Lorentzian fits to the CO ice bands (green and black, respectively) and Gaussian fits to the 2165.7 and 2175.4 cm−1 components of the OCN− band (solid purple and dashed purple, respectively). A dashed red line in the right panels indicates that OCS was not detected, and the Gaussian depth should be regarded as an upper limit.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: IRTF/SpeX spectrum of the MYSO G012.9090-00.2607 (W33A; black solid line) compared to a space-based ISO/SWS spectrum across the full wavelength range (red; Gibb et al. 2004). The IRTF/SpeX and ISO/SWS spectra are overall in good agreement, showing the same absorption features and continuum shape. The dotted line indicates the continuum level described in Section 4.1 and Figures 1–3. The dashed line is the continuum level including absorption by H2O ice, showing the effect of the broad ∼4.5 μm H2O combination mode. A change in slope is visible near ∼5.0 μm in both the IRTF/SpeX and ISO/SWS spectra, due to what appears to be a shallow absorption feature centered on ∼5.25 μm. The change in slope at ∼5.5 μm is due to the onset of the prominent 6.0 μm absorption band. The apparent lack of absorption by gas-phase CO lines in the ISO/SWS spectrum is due to its low spectral resolving power (R = 800 vs. R = 1500).
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Portion of the L-band spectra of the MYSO sample. All targets show the 3.47 μm absorption band, likely caused by NH3 hydrates, and some show signs of hydrocarbon absorption as well near 3.4 μm (e.g., G033.5237). The feature at 3.53 μm is attributed to CH3OH ice. For each target, the left panel shows the adopted local polynomial baseline, and the right panel the baseline subtracted spectrum. In the right panels, the solid green line is a laboratory spectrum of CH3OH ice at a temperature of 10 K (H2O:CH3OH:CO:NH3 = 100:50:1:1; Hudgins et al. 1993), and the dashed green line a Gaussian. The sum of these fits is shown as a solid red line. For targets without a CH3OH ice detection, a dashed red line is shown instead.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption:  M-band spectra of the MYSO sample on optical depth scale. For more details, see the caption of Figure 6.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: Illustration of the removal of gas-phase 12CO rovibrational absorption lines for the MYSO G108.7575−00.9863. Panel (a) is the IRTF/SpeX spectrum before removal, and panel (b) after. Panel (c) shows the rotation diagram used in this process, with E low, N low, and J low, the energy level, column density, and rotational quantum number for the lower energy levels, respectively. Two slope regimes are discerned, which are fitted with two straight lines, corresponding to excitation temperatures of 90 and 895 K and column densities of 7.5 × 1016 and 2.5 × 1017 cm−2, respectively. These temperatures are likely highly inaccurate, and the column densities strongly underestimated due to the lines being optically thick.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: IRTF/SpeX spectra of MYSO sample. For more details, see the caption of Figure 1.
Paper: Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH
Authors: A. C. A. Boogert, K. Brewer, A. Brittain, K. S. Emerson
Figure caption: The OCS ice band toward the sample of MYSOs compared to the same Gaussian, scaled to the best-fit peak optical depth of Table 4 in order to highlight any variations in the sample. The Gaussian represents the best fit to the target G012.9090 (W33A; λ = 4.9012 μm, FWHM = 0.0441 μm).
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Image of the NuSTAR FPMA in Det#1 coordinates. The red thick line indicates the stray light region. The primary source (4U 1954+31) is visible in Det #0 (upper right quadrant).